Wisniewski, John P.; Ge, Jian; Crepp, Justin R.; De Lee, Nathan; Eastman, Jason; Esposito, M.; Fleming, Scott W.; Gaudi, B. Scott; Ghezzi, Luan; Gonzalez-Hernandez, J. I.; Lee, Brian L.; Stassun, Keivan G.; Agol, Eric; Allende-Prieto, C.; Barnes, Rory; Bizyaev, Dmitry; Cargile, Phillip; Chang, Liang; Da Costa, Luiz N.; Porto De Mello, G. F.; Femenía, B.; Ferreira, Leticia D.; Gary, Bruce; Hebb, Leslie; Holtzman, Jon; Liu, Jian; Ma, Bo; Mack, Claude E.; Mahadevan, Suvrath; Maia, Marcio A. G.; Nguyen, Duy Cuong; Ogando, Ricardo L. C.; Oravetz, Daniel J.; Paegert, Martin; Pan, Kaike; Pepper, Joshua; Rebolo, R.; Santiago, Basilio; Schneider, Donald P.; Shelden, Alaina C.; Simmons, Audrey; Tofflemire, Benjamin M.; Wan, Xiaoke; Wang, Ji; Zhao, Bo
Referencia bibliográfica
The Astronomical Journal, Volume 143, Issue 5, article id. 107 (2012).
Fecha de publicación:
5
2012
Número de autores del IAC
5
Número de citas referidas
22
Descripción
TYC 4110-01037-1 has a low-mass stellar companion, whose small mass
ratio and short orbital period are atypical among binary systems with
solar-like (T eff <~ 6000 K) primary stars. Our analysis
of TYC 4110-01037-1 reveals it to be a moderately aged (lsim5 Gyr)
solar-like star having a mass of 1.07 ± 0.08 M &sun;
and radius of 0.99 ± 0.18 R &sun;. We analyze 32
radial velocity (RV) measurements from the SDSS-III MARVELS survey as
well as 6 supporting RV measurements from the SARG spectrograph on the
3.6 m Telescopio Nazionale Galileo telescope obtained over a period of
~2 years. The best Keplerian orbital fit parameters were found to have a
period of 78.994 ± 0.012 days, an eccentricity of 0.1095 ±
0.0023, and a semi-amplitude of 4199 ± 11 m s-1.
We determine the minimum companion mass (if sin i = 1) to be 97.7
± 5.8 M Jup. The system's companion to host star mass
ratio, >=0.087 ± 0.003, places it at the lowest end of
observed values for short period stellar companions to solar-like (T
eff <~ 6000 K) stars. One possible way to create such a
system would be if a triple-component stellar multiple broke up into a
short period, low q binary during the cluster dispersal phase of its
lifetime. A candidate tertiary body has been identified in the system
via single-epoch, high contrast imagery. If this object is confirmed to
be comoving, we estimate it would be a dM4 star. We present these
results in the context of our larger-scale effort to constrain the
statistics of low-mass stellar and brown dwarf companions to FGK-type
stars via the MARVELS survey.
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